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Fig. 9


Comparison of the bolometric light curves of magnetar-powered models RE0p4B4p5o (thick dashed line) and RE0p4B4p5os (thin line) with that inferred for OGLE-SN14-073 (empty circles; Terreran et al. 2017) and SN 1987A (empty squares; Hamuy et al. 1988). The origin of the x−axis is the time of the first signal detection at the outer grid boundary for the models (~4 d after the start of the simulations), or the inferred time of explosion for the observations. We add the magnetar power of these two models (thin dashed line) and the radioactive decay power from 0.07 M of 56 Ni (to match the nebular luminosity of SN 1987A; dash-dotted line). To power the nebular luminosity of OGLE-SN14-073 with radioactive decay requires 0.47 M of 56 Ni (upper dash-dotted line).

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